with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve shows any short peaks
with a total duration of about 35 sec. The peak count rate
was ~3200 counts/sec (15-350 keV), at ~1 sec after the trigger.
The XRT began observing the field at 12:33:24.5 UT, 121.8 seconds after
the BAT trigger. No source was detected in 574 s of promptly downlinked
data, which covered 0% of the BAT error circle. We are waiting for the
full dataset to detect and localise the XRT counterpart.
No UVOT data is available at this time.
We note that this BAT trigger time is within 7 sec of a Fermi-GBM trigger
(trigger= 498141079).
Burst Advocate for this burst is J. L. Racusin (judith.racusin AT nasa.gov).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)

with an uncertainty of 1.7 arcsec (radius, 90% confidence).
UVOT took a settling exposure of 9.8 seconds with the v filter starting 109 seconds after the BAT trigger. We find a source consistent with the position of the afterglow reported by MITSuME (Morita et al GCN Circ 20036) and LCOGT FTS (Guidorzi et al., GCN Circ. 20037). The estimated magnitude is 16.52. No correction has been made for the expected extinction corresponding to E(B-V) of 0.08 in the direction of the burst (Schlegel et al. 1998).

with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 13%.
The mask-weighted light curve shows a complex structure starting at T-10 sec
and ending at T+15 sec. T90 (15-350 keV) is 18.3 +- 2.8 sec (estimated error
including systematics).
The time-averaged spectrum from T-9.1 to T+12.5 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.47 +- 0.15. The fluence in the 15-150 keV band is 1.9 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.10 sec in the 15-150 keV band
is 2.9 +- 0.6 ph/cm2/sec. All the quoted errors are at the 90% confidence
level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/717500/BA/

with an uncertainty of 1.4 arcsec (radius, 90% confidence).
The light curve can be modelled with an initial power-law decay with an
index of alpha=0.45 (+/-0.12), followed by a break at T+1757 s to an
alpha of 1.59 (+0.14, -0.13).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.83 (+0.11, -0.10). The
best-fitting absorption column is 1.5 (+0.9, -0.8) x 10^22 cm^-2, at a
redshift of 2.823, in addition to the Galactic value of 7.5 x 10^20
cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum is 3.7 x
10^-11 (4.5 x 10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:

GCN Circular #20051
E. Bissaldi (Politecnico & INFN Bari)
reports on behalf of the Fermi GBM Team:
"At 12:31:15.91 UT on 14 October 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 161014A (trigger 498141079 / 161014522),
which was also detected by the Swift/BAT (Racusin et al. 2016, GCN 20035).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight at the GBM trigger time is 69 degrees.
The GBM light curve shows multiple peaks with a duration (T90) of
about 37 s (50-300 keV).
The time-averaged spectrum from T0-6 s to T0+23 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.74 +/- 0.09 and
the cutoff energy, parameterized as Epeak, is 167 +/- 15 keV.
The event fluence (10-1000 keV) in this time interval is
(5.4 +/- 0.3)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+7 s in the 10-1000 keV band
is 5.7 +/- 0.3 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."

This source is consistent with the source reported in Morita et al., (GCNs
20036, 20046), Guidorzi et al., (GCN 20037), Xin et al., (GCN
20038), Nakaoka et al., (GCN 20039), Mazaeva et al., (GCN
20042), and Melandri et al., (GCN 20048). These magnitudes are in the AB
system and are not corrected for Galactic extinction in the direction of
the GRB.
We thank the staff of the Observatorio Astron=F3mico Nacional in San Pedro
M=E1rtir.